The ionized gas and nuclear environment in NGC 3783. V. Variability and modeling of the intrinsic ultraviolet absorption

Jack Gabel, Steven B. Kraemer, D. Michael Crenshaw, Ian M. George, W. N. Brandt, Frederick W. Hamann, Mary Elizabeth Kaiser, Shai Kaspi, Gerard A. Kriss, Smita Mathur, Kirpal Nandra, Hagai Netzer, Bradley M. Peterson, Joseph C. Shields, T. J. Turner, Wei Zheng

Research output: Contribution to journalArticle

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Abstract

We present results on the location, physical conditions, and geometry of the outflow in the Seyfert 1 galaxy NGC 3783 from a study of the variable intrinsic UV absorption. Based on analysis of 18 observations with the Space Telescope Imaging Spectrograph on board the Bubble Space Telescope and six observations with the Far Ultraviolet Spectroscopic Explorer obtained between 2000 February and 2002 January, we obtain the following results: (1) The lowest ionization species detected in each of the three strong kinematic components (components 1-3 at radial velocities -1350, -550, and -725 km s-1, respectively) varied, with equivalent widths inversely correlated with the continuum flux. This indicates that the ionization structure in the absorbers responded to changes in the photoionizing flux, with variations occurring over the weekly timescales sampled by our observations. (2) A multicomponent model of the line-of-sight absorption covering factors, which includes an unocculted narrow emission-line region (NLR) and separate covering factors derived for the broad-line region and continuum emission sources, predicts saturation in several lines, consistent with the lack of observed variability in these lines. Differences in covering factors and kinematic structure imply that component 1 is composed of two physically distinct regions (1a and 1b). (3) We obtain column densities for the individual metastable levels from the resolved C III* λ1175 absorption complex in component 1a. Based on our computed metastable level populations, the electron density of this absorber is ∼3 × 104 cm-3. Combined with photoionization modeling results, this places component 1 a at ∼25 pc from the central source. (4) Using time-dependent calculations, we are able to reproduce the detailed variability observed in component 1 and derive upper limits on the distances for components 2 and 3 of ≤25 and ≤50 pc, respectively. (5) The ionization parameters derived for the higher ionization UV absorbers (components 1b, 2, and 3 with log U ≈ -0.5) are consistent with the modeling results for the lowest ionization X-ray component, but with smaller total column density. The high-ionization UV components are found to have pressures similar to those of the three X-ray ionization components. These results are consistent with an inhomogeneous wind model for the outflow in NGC 3783, with denser, colder, lower ionization regions embedded in more highly ionized gas. (6) Based on the predicted emission-line luminosities, global covering factor constraints, and distances derived for the UVabsorbers, they may be identified with emission-line gas observed in the inner NLR of AGNs. We explore constraints for dynamical models of AGN outflows implied by these results.

Original languageEnglish
Pages (from-to)741-761
Number of pages21
JournalAstrophysical Journal
Volume631
Issue number2 I
DOIs
StatePublished - Oct 1 2005
Externally publishedYes

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ultraviolet absorption
ionized gases
ionization
gas
modeling
outflow
coverings
absorbers
kinematics
telescopes
continuums
electron density
bubble
saturation
radial velocity
line of sight
timescale
spectrographs
geometry
photoionization

All Science Journal Classification (ASJC) codes

  • Space and Planetary Science
  • Nuclear and High Energy Physics

Cite this

Gabel, J., Kraemer, S. B., Crenshaw, D. M., George, I. M., Brandt, W. N., Hamann, F. W., ... Zheng, W. (2005). The ionized gas and nuclear environment in NGC 3783. V. Variability and modeling of the intrinsic ultraviolet absorption. Astrophysical Journal, 631(2 I), 741-761. https://doi.org/10.1086/432682

The ionized gas and nuclear environment in NGC 3783. V. Variability and modeling of the intrinsic ultraviolet absorption. / Gabel, Jack; Kraemer, Steven B.; Crenshaw, D. Michael; George, Ian M.; Brandt, W. N.; Hamann, Frederick W.; Kaiser, Mary Elizabeth; Kaspi, Shai; Kriss, Gerard A.; Mathur, Smita; Nandra, Kirpal; Netzer, Hagai; Peterson, Bradley M.; Shields, Joseph C.; Turner, T. J.; Zheng, Wei.

In: Astrophysical Journal, Vol. 631, No. 2 I, 01.10.2005, p. 741-761.

Research output: Contribution to journalArticle

Gabel, J, Kraemer, SB, Crenshaw, DM, George, IM, Brandt, WN, Hamann, FW, Kaiser, ME, Kaspi, S, Kriss, GA, Mathur, S, Nandra, K, Netzer, H, Peterson, BM, Shields, JC, Turner, TJ & Zheng, W 2005, 'The ionized gas and nuclear environment in NGC 3783. V. Variability and modeling of the intrinsic ultraviolet absorption', Astrophysical Journal, vol. 631, no. 2 I, pp. 741-761. https://doi.org/10.1086/432682
Gabel, Jack ; Kraemer, Steven B. ; Crenshaw, D. Michael ; George, Ian M. ; Brandt, W. N. ; Hamann, Frederick W. ; Kaiser, Mary Elizabeth ; Kaspi, Shai ; Kriss, Gerard A. ; Mathur, Smita ; Nandra, Kirpal ; Netzer, Hagai ; Peterson, Bradley M. ; Shields, Joseph C. ; Turner, T. J. ; Zheng, Wei. / The ionized gas and nuclear environment in NGC 3783. V. Variability and modeling of the intrinsic ultraviolet absorption. In: Astrophysical Journal. 2005 ; Vol. 631, No. 2 I. pp. 741-761.
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abstract = "We present results on the location, physical conditions, and geometry of the outflow in the Seyfert 1 galaxy NGC 3783 from a study of the variable intrinsic UV absorption. Based on analysis of 18 observations with the Space Telescope Imaging Spectrograph on board the Bubble Space Telescope and six observations with the Far Ultraviolet Spectroscopic Explorer obtained between 2000 February and 2002 January, we obtain the following results: (1) The lowest ionization species detected in each of the three strong kinematic components (components 1-3 at radial velocities -1350, -550, and -725 km s-1, respectively) varied, with equivalent widths inversely correlated with the continuum flux. This indicates that the ionization structure in the absorbers responded to changes in the photoionizing flux, with variations occurring over the weekly timescales sampled by our observations. (2) A multicomponent model of the line-of-sight absorption covering factors, which includes an unocculted narrow emission-line region (NLR) and separate covering factors derived for the broad-line region and continuum emission sources, predicts saturation in several lines, consistent with the lack of observed variability in these lines. Differences in covering factors and kinematic structure imply that component 1 is composed of two physically distinct regions (1a and 1b). (3) We obtain column densities for the individual metastable levels from the resolved C III* λ1175 absorption complex in component 1a. Based on our computed metastable level populations, the electron density of this absorber is ∼3 × 104 cm-3. Combined with photoionization modeling results, this places component 1 a at ∼25 pc from the central source. (4) Using time-dependent calculations, we are able to reproduce the detailed variability observed in component 1 and derive upper limits on the distances for components 2 and 3 of ≤25 and ≤50 pc, respectively. (5) The ionization parameters derived for the higher ionization UV absorbers (components 1b, 2, and 3 with log U ≈ -0.5) are consistent with the modeling results for the lowest ionization X-ray component, but with smaller total column density. The high-ionization UV components are found to have pressures similar to those of the three X-ray ionization components. These results are consistent with an inhomogeneous wind model for the outflow in NGC 3783, with denser, colder, lower ionization regions embedded in more highly ionized gas. (6) Based on the predicted emission-line luminosities, global covering factor constraints, and distances derived for the UVabsorbers, they may be identified with emission-line gas observed in the inner NLR of AGNs. We explore constraints for dynamical models of AGN outflows implied by these results.",
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T1 - The ionized gas and nuclear environment in NGC 3783. V. Variability and modeling of the intrinsic ultraviolet absorption

AU - Gabel, Jack

AU - Kraemer, Steven B.

AU - Crenshaw, D. Michael

AU - George, Ian M.

AU - Brandt, W. N.

AU - Hamann, Frederick W.

AU - Kaiser, Mary Elizabeth

AU - Kaspi, Shai

AU - Kriss, Gerard A.

AU - Mathur, Smita

AU - Nandra, Kirpal

AU - Netzer, Hagai

AU - Peterson, Bradley M.

AU - Shields, Joseph C.

AU - Turner, T. J.

AU - Zheng, Wei

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N2 - We present results on the location, physical conditions, and geometry of the outflow in the Seyfert 1 galaxy NGC 3783 from a study of the variable intrinsic UV absorption. Based on analysis of 18 observations with the Space Telescope Imaging Spectrograph on board the Bubble Space Telescope and six observations with the Far Ultraviolet Spectroscopic Explorer obtained between 2000 February and 2002 January, we obtain the following results: (1) The lowest ionization species detected in each of the three strong kinematic components (components 1-3 at radial velocities -1350, -550, and -725 km s-1, respectively) varied, with equivalent widths inversely correlated with the continuum flux. This indicates that the ionization structure in the absorbers responded to changes in the photoionizing flux, with variations occurring over the weekly timescales sampled by our observations. (2) A multicomponent model of the line-of-sight absorption covering factors, which includes an unocculted narrow emission-line region (NLR) and separate covering factors derived for the broad-line region and continuum emission sources, predicts saturation in several lines, consistent with the lack of observed variability in these lines. Differences in covering factors and kinematic structure imply that component 1 is composed of two physically distinct regions (1a and 1b). (3) We obtain column densities for the individual metastable levels from the resolved C III* λ1175 absorption complex in component 1a. Based on our computed metastable level populations, the electron density of this absorber is ∼3 × 104 cm-3. Combined with photoionization modeling results, this places component 1 a at ∼25 pc from the central source. (4) Using time-dependent calculations, we are able to reproduce the detailed variability observed in component 1 and derive upper limits on the distances for components 2 and 3 of ≤25 and ≤50 pc, respectively. (5) The ionization parameters derived for the higher ionization UV absorbers (components 1b, 2, and 3 with log U ≈ -0.5) are consistent with the modeling results for the lowest ionization X-ray component, but with smaller total column density. The high-ionization UV components are found to have pressures similar to those of the three X-ray ionization components. These results are consistent with an inhomogeneous wind model for the outflow in NGC 3783, with denser, colder, lower ionization regions embedded in more highly ionized gas. (6) Based on the predicted emission-line luminosities, global covering factor constraints, and distances derived for the UVabsorbers, they may be identified with emission-line gas observed in the inner NLR of AGNs. We explore constraints for dynamical models of AGN outflows implied by these results.

AB - We present results on the location, physical conditions, and geometry of the outflow in the Seyfert 1 galaxy NGC 3783 from a study of the variable intrinsic UV absorption. Based on analysis of 18 observations with the Space Telescope Imaging Spectrograph on board the Bubble Space Telescope and six observations with the Far Ultraviolet Spectroscopic Explorer obtained between 2000 February and 2002 January, we obtain the following results: (1) The lowest ionization species detected in each of the three strong kinematic components (components 1-3 at radial velocities -1350, -550, and -725 km s-1, respectively) varied, with equivalent widths inversely correlated with the continuum flux. This indicates that the ionization structure in the absorbers responded to changes in the photoionizing flux, with variations occurring over the weekly timescales sampled by our observations. (2) A multicomponent model of the line-of-sight absorption covering factors, which includes an unocculted narrow emission-line region (NLR) and separate covering factors derived for the broad-line region and continuum emission sources, predicts saturation in several lines, consistent with the lack of observed variability in these lines. Differences in covering factors and kinematic structure imply that component 1 is composed of two physically distinct regions (1a and 1b). (3) We obtain column densities for the individual metastable levels from the resolved C III* λ1175 absorption complex in component 1a. Based on our computed metastable level populations, the electron density of this absorber is ∼3 × 104 cm-3. Combined with photoionization modeling results, this places component 1 a at ∼25 pc from the central source. (4) Using time-dependent calculations, we are able to reproduce the detailed variability observed in component 1 and derive upper limits on the distances for components 2 and 3 of ≤25 and ≤50 pc, respectively. (5) The ionization parameters derived for the higher ionization UV absorbers (components 1b, 2, and 3 with log U ≈ -0.5) are consistent with the modeling results for the lowest ionization X-ray component, but with smaller total column density. The high-ionization UV components are found to have pressures similar to those of the three X-ray ionization components. These results are consistent with an inhomogeneous wind model for the outflow in NGC 3783, with denser, colder, lower ionization regions embedded in more highly ionized gas. (6) Based on the predicted emission-line luminosities, global covering factor constraints, and distances derived for the UVabsorbers, they may be identified with emission-line gas observed in the inner NLR of AGNs. We explore constraints for dynamical models of AGN outflows implied by these results.

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